Growth and Characterisation of Radio Frequency Magnetron Sputttered Indium Tin Oxide Thin Films

The increasing interest in the interaction of light with electricity and electronically active materials made the materials and techniques for producing semitransparent electrically conducting films particularly attractive. Transparent conductors have found major applications in a number of electronic and optoelectronic devices including resistors, transparent heating elements, antistatic and electromagnetic shield coatings, transparent electrode for solar cells, antireflection coatings, heat reflecting mirrors in glass windows and many other. Tin doped indium oxide (indium tin oxide or ITO) is one of the most commonly used transparent conducting oxides. At present and likely well into the future this material offers best available performance in terms of conductivity and transmittivity combined with excellent environmental stability, reproducibility and good surface morphology. Although partial transparency, with a reduction in conductivity, can be obtained for very thin metallic films, high transparency and simultaneously high conductivity cannot be attained in intrinsic stoichiometric materials. The only way this can be achieved is by creating electron degeneracy in a wide bandgap (Eg > 3eV or more for visible radiation) material by controllably introducing non-stoichiometry and/or appropriate dopants. These conditions can be conveniently met for ITO as well as a number of other materials like Zinc oxide, Cadmium oxide etc. ITO shows interesting and technologically important combination of properties viz high luminous transmittance, high IR reflectance, good electrical conductivity, excellent substrate adherence and chemical inertness. ITO is a key part of solar cells, window coatings, energy efficient buildings, and flat panel displays. In solar cells, ITO can be the transparent, conducting top layer that lets light into the cell to shine the junction and lets electricity flow out. Improving the ITO layer can help improve the solar cell efficiency. A transparent ii conducting oxide is a material with high transparency in a derived part of the spectrum and high electrical conductivity. Beyond these key properties of transparent conducting oxides (TCOs), ITO has a number of other key characteristics. The structure of ITO can be amorphous, crystalline, or mixed, depending on the deposition temperature and atmosphere. The electro-optical properties are a function of the crystallinity of the material. In general, ITO deposited at room temperature is amorphous, and ITO deposited at higher temperatures is crystalline. Depositing at high temperatures is more expensive than at room temperature, and this method may not be compatible with the underlying devices. The main objective of this thesis work is to optimise the growth conditions of Indium tin oxide thin films at low processing temperatures. The films are prepared by radio frequency magnetron sputtering under various deposition conditions. The films are also deposited on to flexible substrates by employing bias sputtering technique. The films thus grown were characterised using different tools. A powder x-ray diffractometer was used to analyse the crystalline nature of the films. The energy dispersive x-ray analysis (EDX) and scanning electron microscopy (SEM) were used for evaluating the composition and morphology of the films. Optical properties were investigated using the UVVIS- NIR spectrophotometer by recording the transmission/absorption spectra. The electrical properties were studied using vander Pauw four probe technique. The plasma generated during the sputtering of the ITO target was analysed using Langmuir probe and optical emission spectral studies.

Determination of charge carrier transport in radio frequency plasma polymerized aniline thin films

The carrier transport mechanism of polyaniline (PA) thin films prepared by radio frequency plasma polymerization is described in this paper. The mechanism of electrical conduction and carrier mobility of PA thin films for different temperatures were examined using the aluminium–PA–aluminium (Al–PA–Al) structure. It is found that the mechanism of carrier transport in these thin films is space charge limited conduction. J –V studies on an asymmetric electrode configuration using indium tin oxide (ITO) as the base electrode and Al as the upper electrode (ITO–PA–Al structure) show a diode-like behaviour with a considerable rectification ratio

Hints for a fast precessing relativistic radio jet in LS I + 61° 303

Here we discuss two consecutive MERLIN observations of the X-ray binary LS I +61° 303 . The first observation shows a double-sided jet extending up to about 200 AU on both sides of a central source. The jet shows a bent S-shaped structure similar to the one displayed by the well-known precessing jet of SS 433 . The precession suggested in the first MERLIN image becomes evident in the second one, showing a one-sided bent jet significantly rotated with respect to the jet of the day before. We conclude that the derived precession of the relativistic (beta=0.6) jet explains puzzling previous VLBI results. Moreover, the fact that the precession is fast could be the explanation of the never understood short term (days) variability of the associated gamma-ray source 2CG 135+01 / 3EG J0241+6103

The determinants of competitive success in the interwar British radio industry

This article discusses the sources of competitive advantage in the interwar British radio industry. Specifically, it examines why sections of the industry that reaped substantial monopoly rents from the downstream value chain failed to dominate the industry. During the 1920s Marconi (which controlled the fundamental UK patents) had a key cost advantage, as had other members of the ‘Big Six’ electrical engineering firms which formed the BBC and were granted preferential royalties. Meanwhile the valve manufacturers' cartel was also able to extract high rents from set manufacturers. The vertical integration literature suggests that input monopolists have incentives to control downstream production. Yet—in contrast to the gramophone industry, which became concentrated into two huge companies following market saturation in the 1930s—radio retained a much more competitive structure. The Big Six failed to capitalize fully on their initial cost advantages owing to logistical weaknesses in supplying markets subject to rapid technical and design obsolescence. Subsequently, during the 1930s, marketing innovations are shown to have played a key role in allowing several independents to establish successful brands. This gave them sufficient scale to provide strong bargaining positions with input suppliers, negating most of their initial cost disadvantage.

Particle acceleration and magnetic field structure in PKS 2155-304: optical polarimetric observations

In this paper, we present multiband optical polarimetric observations of the very-high energy blazar PKS 2155-304 made simultaneously with a HESS/Fermi high-energy campaign in 2008, when the source was found to be in a low state. The intense daily coverage of the data set allowed us to study in detail the temporal evolution of the emission, and we found that the particle acceleration time-scales are decoupled from the changes in the polarimetric properties of the source. We present a model in which the optical polarimetric emission originates at the polarized mm-wave core and propose an explanation for the lack of correlation between the photometric and polarimetric fluxes. The optical emission is consistent with an inhomogeneous synchrotron source in which the large-scale field is locally organized by a shock in which particle acceleration takes place. Finally, we use these optical polarimetric observations of PKS 2155-304 at a low state to propose an origin for the quiescent gamma-ray flux of the object, in an attempt to provide clues for the source of its recently established persistent TeV emission.

Effects of thermal annealing on the semi-insulating properties of radio frequency magnetron sputtering-produced germanate thin films

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Informative Radio Models in Brazil: The All-News Networks

This study analyzes the particularities of Brazilian radio networks that adopt the all-news format and briefly presents the main national and international experiences for the implementation of the model and its conceptualization. Besides the bibliographic review, we use the multiple-case study, analyzing as the empirical objects CBN and BandNews FM networks. Also, we apply methodological procedures of systematic non-participant observation, supplemented by interviews and surveys. We conclude that the different all-news programming models and network organizations influence the processes of production, information structure, broadcasting language, and therefore the stations' profile. © 2011 Copyright Taylor and Francis Group, LLC.

Effects of substrate temperature, substrate orientation, and energetic atomic collisions on the structure of GaN films grown by reactive sputtering

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Magnetic fields around radio galaxies from Faraday rotation measure analysis

The purpose of this thesis is to investigate the strength and structure of the magnetized medium surrounding radio galaxies via observations of the Faraday effect. This study is based on an analysis of the polarization properties of radio galaxies selected to have a range of morphologies (elongated tails, or lobes with small axial ratios) and to be located in a variety of environments (from rich cluster core to small group). The targets include famous objects like M84 and M87. A key aspect of this work is the combination of accurate radio imaging with high-quality X-ray data for the gas surrounding the sources. Although the focus of this thesis is primarily observational, I developed analytical models and performed two- and three-dimensional numerical simulations of magnetic fields. The steps of the thesis are: (a) to analyze new and archival observations of Faraday rotation measure (RM) across radio galaxies and (b) to interpret these and existing RM images using sophisticated two and three-dimensional Monte Carlo simulations. The approach has been to select a few bright, very extended and highly polarized radio galaxies. This is essential to have high signal-to-noise in polarization over large enough areas to allow computation of spatial statistics such as the structure function (and hence the power spectrum) of rotation measure, which requires a large number of independent measurements. New and archival Very Large Array observations of the target sources have been analyzed in combination with high-quality X-ray data from the Chandra, XMM-Newton and ROSAT satellites. The work has been carried out by making use of: 1) Analytical predictions of the RM structure functions to quantify the RM statistics and to constrain the power spectra of the RM and magnetic field. 2) Two-dimensional Monte Carlo simulations to address the effect of an incomplete sampling of RM distribution and so to determine errors for the power spectra. 3) Methods to combine measurements of RM and depolarization in order to constrain the magnetic-field power spectrum on small scales. 4) Three-dimensional models of the group/cluster environments, including different magnetic field power spectra and gas density distributions. This thesis has shown that the magnetized medium surrounding radio galaxies appears more complicated than was apparent from earlier work. Three distinct types of magnetic-field structure are identified: an isotropic component with large-scale fluctuations, plausibly associated with the intergalactic medium not affected by the presence of a radio source; a well-ordered field draped around the front ends of the radio lobes and a field with small-scale fluctuations in rims of compressed gas surrounding the inner lobes, perhaps associated with a mixing layer.

From Radio Channel Modeling to a System Level Perspective in Body-Centric Communications

Body-centric communications are emerging as a new paradigm in the panorama of personal communications. Being concerned with human behaviour, they are suitable for a wide variety of applications. The advances in the miniaturization of portable devices to be placed on or around the body, foster the diffusion of these systems, where the human body is the key element defining communication characteristics. This thesis investigates the human impact on body-centric communications under its distinctive aspects. First of all, the unique propagation environment defined by the body is described through a scenario-based channel modeling approach, according to the communication scenario considered, i.e., on- or on- to off-body. The novelty introduced pertains to the description of radio channel features accounting for multiple sources of variability at the same time. Secondly, the importance of a proper channel characterisation is shown integrating the on-body channel model in a system level simulator, allowing a more realistic comparison of different Physical and Medium Access Control layer solutions. Finally, the structure of a comprehensive simulation framework for system performance evaluation is proposed. It aims at merging in one tool, mobility and social features typical of the human being, together with the propagation aspects, in a scenario where multiple users interact sharing space and resources.

Radio-holografía de microondas para la optimización de la superficie de grandes antenas reflectoras

En el presente trabajo de tesis se afronta el problema de la optimización de la superficie de grandes antenas reflectoras. Es sabido que los grandes reflectores, formados por una superficie panelada, sufren deformaciones debidas al impacto del viento, a los cambios de temperatura y a los efectos gravitacionales derivados del gran peso de la estructura. Estos efectos hacen que los reflectores pierdan su forma ideal, generalmente de paraboloide, y se reduzca su eficiencia de apertura y, por tanto, se limite la máxima frecuencia de uso de los mismos. Es necesario, por tanto, disponer de técnicas que permitan medir el estado de la superficie de grandes reflectores, y derivar los ajustes necesarios a aplicar sobre los tornillos de soporte de cada uno de los paneles que conforman dicha superficie. De esta manera, se devolvería al reflector su forma óptima y aumentaría la eficiencia de apertura y el rango de frecuencias de uso. Hay que resaltar que el aumento de la eficiencia de un radiotelescopio supone una reducción en el tiempo de integración necesario para la detección de las debilísimas señales generadas por las radiofuentes naturales, ahorrando así valioso tiempo de observación. Además, el incremento en el rango de frecuencias permite la detección de nuevas líneas o especies moleculares en dichas radiofuentes. Tras un primer capítulo introductorio, se presenta, en el capítulo segundo, la geometría de estos grandes reflectores y la influencia de los distintos factores que afectan a la calidad de la superficie de los mismos, como la gravedad, el viento y la temperatura, particularizando para el caso del radiotelescopio de 40 metros del Centro Astronómico de Yebes. En el tercer capítulo, se presentan las diferentes técnicas metrológicas empleadas actualmente para abordar la determinación de estos ajustes, mostrándose las ventajas e inconvenientes de cada una de ellas. Actualmente, la técnica metrológica más precisa y rápida para llevar a cabo esta tarea de caracterización de la superficie de un gran reflector, es la radio-holografía de microondas presentada en el capítulo cuarto. A partir de las medidas proporcionadas por esta técnica, realizadas con la ayuda de un transmisor, y mediante transformaciones de campo, se calculan los errores de la superficie del reflector, respecto al paraboloide ideal, y se derivan los ajustes necesarios. En los capítulos quinto y sexto se presentan los resultados de la aplicación de esta técnica a dos radiotelescopios: el de 30 metros de IRAM en Pico de Veleta (Granada) y los prototipos de 12 metros de las antenas del proyecto ALMA. Por su parte, el capítulo séptimo contiene el núcleo fundamental de esta tesis y presenta el desarrollo de la técnica de radio-holografía de microondas para optimizar la superficie del radiotelescopio de 40 metros del Centro Astronómico de Yebes. Para ello, ha sido necesario diseñar, construir e instalar un receptor de doble canal en banda Ku en foco primario, y la instrumentación asociada para hacer las medidas de amplitud y fase del diagrama de radiación. Además, ha sido necesario desarrollar el software para llevar a cabo las transformaciones de campo y derivar los ajustes de los paneles. De las medidas holográficas iniciales resultó un error de la superficie del radiotelescopio de 485 μm WRMS, respecto al paraboloide ideal en dirección normal. Tras varias iteraciones del proceso de medida y ajuste, se consiguió reducir dicho error a 194 μm WRMS. Esta notable mejora de la calidad de la superficie ha supuesto aumentar la eficiencia de apertura desde 2,6% al 38,2% a 86 GHz, para un receptor a esta frecuencia situado en el foco primario que produjese la misma iluminación que el receptor de holografía. In this thesis the problem of large reflector antenna surface optimization is faced. It is well known that large reflectors, which are made of a panelled surface, suffer from deformations due to the impact of wind, temperature gradients and gravity loads coming from the high weigth of the structure. These effects distort the ideal reflector shape, which is a paraboloid in most cases, hence reducing the aperture efficiency of the reflector and limiting the maximum frequency of operation. Therefore, it is necessary to have some techniques to measure the status of large reflector surfaces and to derive the adjustment values to be applied to the screws that connect the surface panels to the reflector back-up structure. In this way, the reflector would recover its optimum shape and the aperture efficiency and frequency range would increase. It has to be stated that an increment in the radiotelescope aperture efficiency would imply a reduction in the integration time needed to detect such weak signals coming from natural radiosources in space and, hence, an important saving in observation time. In addition, the increase in the frequency range of operation would allow the detection of new molecular lines in those radiosources. After the introduction, the second chapter shows the geometry of large reflector antennas and the impact on its surface quality of different factors like gravity, wind and temperature, particularly for the case of the Centro Astronómico de Yebes 40 meter radiotelescope. The third chapter deals with the different metrology techniques used to determine the panel adjustments, including the advantages and drawbacks of each one Currently, the most accurate and fast metrologic technique to carry out the characterization of large reflector surfaces is microwave radio-holography2, which is shown in chapter four. From the measurements provided by microwave radio-holography, performed with the help of a transmitter, and with the use of field transformations, the reflector surface errors are computed and the panel adjustments are derived. Chapters five and six show the results of holographic measurements applied to two first class radiotelescopes: the IRAM 30 meter radiotelescope and the 12 meter prototype antennas for the ALMA project. Chapter seven contains the main work of this thesis. It presents the development of the microwave radio-holography technique for the optimization of the Centro Astronómico de Yebes 40m radiotelescope. The work implied the design, construction and instalation of a prime focus Ku-band dual channel receiver, together with the associated instrumentation to measure the amplitude and phase of the radiotelescope radiation pattern. In addition, the software to carry out field transformations and screw settings computations was developed too. Initial holography measurements came up with an surface error of 485 μmWRMS in normal direction with respect to the best-fit paraboloid. After a few iterations of the measurementadjustment cycle, the surface error was reduced to 194 μm WRMS. This remarkable improvement in surface quality means an increment in aperture efficiency from 2,6% to 38,2% at 86 GHz, assuming a receiver at this frequency in prime focus position which produces the same illumination as the holography receiver.

Radio-echo sounding and ice volume estimates of western Nordenskiöld Land glaciers, Svalbard

As part of ongoing work to obtain a reliable estimate of the total ice volume of Svalbard glaciers and their potential contribution to sea-level rise, we present here volume calculations, with detailed error estimates, for ten glaciers on western Nordenskiöld Land, central Spitsbergen, Svalbard. The volume estimates are based upon a dense net of GPR-retrieved ice thickness data collected over several field campaigns spanning the period 1999-2012. On the basis of the pattern of scattering in theradargrams, we also analyse the hydrothermal structure of these glaciers.

Subparsec-scale structure and evolution of Centaurus A (NGC5128).

We present a series of 8.4-GHz very-long-baseline radio interferometry images of the nucleus of Centaurus A (NGC5128) made with a Southern Hemisphere array, representing a 3.3-year monitoring effort. The nuclear radio jet is approximately 50 milliarcseconds in extent, or at the 3.5-megaparsec distance of NGC5128, approximately 1 parsec in length. Subluminal motion is seen and structural changes are observed on time scales shorter than 4 months. High-resolution observations at 4.8 and 8.4 GHz made in November 1992 reveal a complex morphology and allow us to unambiguously identify the self-absorbed core located at the southwestern end of the jet.

Very-long-baseline radio interferometry (VLBI) observations of gamma-ray blazars: results from millimeter-VLBI observations.

VLBI observations of the extremely gamma-bright blazar PKS 0528+134 at 8, 22, 43, and 86 GHz reveal a strongly bent one-sided-core jet structure with at least three moving and two apparently stationary jet components. At the highest observing frequencies the brightest and most compact jet component (the VLBI core) is unresolved with an upper limit to its size of approximately 50 microarcsec corresponding to approximately 0.2 parsec [H0 = 100 km.s-1.Mpc-1 (megaparsec-1), q0 = 0.5, where H0 is Hubble constant and q0 is the deceleration parameter]. Two 86-GHz VLBI observations performed in 1993.3 and 1994.0 reveal a new jet component emerging with superluminal speed from the core. Linear back-extrapolation of its motion yields strong evidence that the ejection of this component is related to an outburst in the millimeter regime and a preceding intense flare of the gamma-flux density observed in early 1993. This and the radio/optical "light curves" and VLBI data for two other sources (S5 0836+710 and 3C 454.3) suggest that the observed gamma-radiation might be Doppler-boosted and perhaps is closely related to the physical processes acting near the "base" of the highly relativistic jets observed in quasars.